For example, consider the analysis of Drischler et al. [1]}, who extrapolate up from
\(n_{\rm sat}\)  using chiral effective field theory.
To obtain neutron stars with masses above two solar masses, they find that there is a region of density
in which the EoS is stiff: if there is a neutron star of \(2.6\)  solar masses,
at some \(n_B\) , \(c_s^2 \sim 0.55\) .
To agree with small tidal deformability from GW170817, though, the EoS of nuclear matter must be soft until
\(n_B \sim 1.5 - 1.8 n_{\rm sat}\) .
